Far Infrared mapping of NGC 891

Popescu, Cristina; Tuffs, R.; Kylafis, N. D.; Madore, Barry F.

doi:10.1051/0004-6361:20031581

Cited by 66 publications

(70 citation statements)

References 36 publications

(41 reference statements)

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“…This component was needed to account for the amplitude of the submm emission. Strong support for the reality of the elements of the model of Popescu et al (2000) comes not only from the success of the model to fit the integrated SED, but also from the good agreement between the observed surface brightness distributions in the FIR and those predicted by the model (Popescu et al 2004). Additional support is provided by the ability to predict UV magnitudes, as shown in this paper.…”

Section: Introductionmentioning

confidence: 87%

“…Another result to emerge from this work was that the old stellar populations have scaleheights larger than those of the associated dust. The resulting parameters for NGC 891, derived independently at each optical/NIR wavelength by Xilouris et al (1999), were used in Paper I for the modelling of the UV-submm SED of this galaxy and were found to be consistent with the FIR morphology of NGC 891 (Popescu et al 2004). Therefore we adopt these parameters in this work, taking their averages over the optical/NIR range, since no trend with wavelength is apparent.…”

Section: The Diffuse Componentmentioning

confidence: 95%

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Modelling the spectral energy distribution of galaxies

Tuffs

Popescu

Völk

et al. 2004

A&A

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232

428

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Abstract. We present new calculations of the attenuation of stellar light from spiral galaxies using geometries for stars and dust which can reproduce the entire spectral energy distribution from the ultraviolet (UV) to the Far-infrared (FIR)/submillimeter (submm) and can also account for the surface brightness distribution in both the optical/Near-infrared (NIR) and FIR/submm. The calculations are based on the model of Popescu et al. (2000), which incorporates a dustless stellar bulge, a disk of old stars with associated diffuse dust, a thin disk of young stars with associated diffuse dust, and a clumpy dust component associated with star-forming regions in the thin disk. The attenuations, which incorporate the effects of multiple anisotropic scattering, are derived separately for each stellar component, and presented in the form of easily accessible polynomial fits as a function of inclination, for a grid in optical depth and wavelength. The wavelength range considered is between 912 Å and 2.2 µm, sampled such that attenuation can be conveniently calculated both for the standard optical bands and for the bands covered by GALEX. The attenuation characteristics of the individual stellar components show marked differences between each other. A general formula is given for the calculation of composite attenuation, valid for any combination of the bulge-to-disk ratio and amount of clumpiness. As an example, we show how the optical depth derived from the variation of attenuation with inclination depends on the bulge-to-disk ratio. Finally, a recipe is given for a self-consistent determination of the optical depth from the Hα/Hβ line ratio.

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Section: Introductionmentioning

confidence: 87%

Section: The Diffuse Componentmentioning

confidence: 95%

Modelling the spectral energy distribution of galaxies

Tuffs

Popescu

Völk

et al. 2004

A&A

Self Cite

232

428

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show abstract

“…The physical quantities assumed in the simulations are tied to the case of NGC 891, an Sb-type edge-on galaxy whose SED and surface brightness distributions have been the subject of extensive studies (Xilouris et al 1999;Popescu et al 2000Popescu et al , 2004Alton et al 2004;Dasyra et al 2005). In accordance with these works, a distance of 9.5 Mpc is assumed.…”

Section: An Application: Ngc 891mentioning

confidence: 99%

Dust extinction and emission in a clumpy galactic disk

Bianchi¹

2008

A&A

116

201

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Aims. I present the Monte Carlo radiative transfer code TRADING (Transfer of RAdiation through Dust In Galaxies). The code selfconsistently computes the extinction of radiation in a dusty medium (including absorption and scattering) and the dust emission. Methods. A binary-tree adaptive grid is used for the description of the dust distribution. Dust radiation is computed at thermal equilibrium or under stochastic heating conditions, for a distribution of grains of different radii and materials. The code is applied to the case of a clumpy galactic disk, including both diffuse dust and a distribution of spherical clouds modelled on the GMCs of local galaxies. Diffuse and localised sources of starlight are used, with independent spectra. Results. A model is provided for the edge-on galaxy NGC 891. The SED of the galaxy from the UV to the submm/mm range can be well reproduced by a bulge/disk configuration of old stars together with an extended dust disk, as suggested by the analysis of optical/near-infrared images; a clumpy dust distribution of the same mass as the diffuse dust disk, together with a UV emitting component, half of which is in the form of a diffuse disk and half in sources embedded in clouds. In total, it is found that about 35% of the bolometric radiation is absorbed (and emitted) by dust; that absorption of starlight from the old population contributes to about 60% of the dust emission. A significant component of the dust emission from clouds is due to absorption of diffuse radiation. Radial profiles of dust emission in a clumpy disk are almost independent of the wavelength, with the exception of the wavelength range on the Wien side of the thermal equilibrium peak.

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“…It is classified as an Sb galaxy in the Third Reference Catalogue of Bright Galaxies (de Vaucouleurs et al 1991), but there is evidence at multiple wavelengths for a bar (e.g., Sofue & Nakai 1993;Garcia-Burillo & Guelin 1995;Schechtman-Rook & Bershady 2013). Due to similarities in mass, morphology, and bolometric luminosity, NGC 891 is often considered a Milky Way analog (van der Kruit 1984); however, the far-infrared star formation rate is somewhat higher in the former at 3.8 M ⊙ yr −1 (Popescu et al 2004). There is evidence in the HII region number density as well as the far-infrared and radio emission morphology that the star formation rate is highest in the northeast side of the disk (e.g., Wainscoat et al 1987;Dettmar 1990).…”

Section: Introductionmentioning

confidence: 99%

Testing a Dynamical Equilibrium Model of the Extraplanar Diffuse Ionized Gas in NGC 891

Boettcher

Zweibel

Gallagher

et al. 2016

ApJ

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The observed scale heights of extraplanar diffuse ionized gas (eDIG) layers exceed their thermal scale heights by a factor of a few in the Milky Way and other nearby edge-on disk galaxies. Here, we test a dynamical equilibrium model of the extraplanar diffuse ionized gas layer in NGC 891, where we ask whether the thermal, turbulent, magnetic field, and cosmic ray pressure gradients are sufficient to support the layer. In optical emission line spectroscopy from the SparsePak integral field unit on the WIYN 3.5-meter telescope, the Hα emission in position-velocity space suggests that the eDIG is found in a ring between galactocentric radii of R min ≤ R ≤ 8 kpc, where R min ≥ 2 kpc. We find that the thermal (σ th = 11 km s −1 ) and turbulent (σ turb = 25 km s −1 ) velocity dispersions are insufficient to satisfy the hydrostatic equilibrium equation given an exponential electron scale height of h z = 1.0 kpc. Using a literature analysis of radio continuum observations from the CHANG-ES survey, we demonstrate that the magnetic field and cosmic ray pressure gradients are sufficient to stably support the gas at R ≥ 8 kpc if the cosmic rays are sufficiently coupled to the system (γ cr = 1.45). Thus, a stable dynamical equilibrium model is viable only if the extraplanar diffuse ionized gas is found in a thin ring around R = 8 kpc, and non-equilibrium models such as a galactic fountain flow are of interest for further study.

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Far Infrared mapping of NGC 891

Cited by 66 publications

References 36 publications

Modelling the spectral energy distribution of galaxies

Modelling the spectral energy distribution of galaxies

Dust extinction and emission in a clumpy galactic disk

Testing a Dynamical Equilibrium Model of the Extraplanar Diffuse Ionized Gas in NGC 891

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